adsabs/AstroCLIMB huggingface dataset:
Paper: Deep Learning Based Solar Flare Forecasting Model. II. Influence of Image Resolution
Authors: Sixuan Liu, Long Xu, Zhongrui Zhao, R. Erdélyi, Marianna B. Korsós, Xin Huang
Figure caption: AlexNet structure. AlexNet contains eight layers. Blue rectangle denotes operations and layers. Among them, “Conv” stands for convolution layer, “Max pool” stands for overlapping max-pooling operation, “FC” stands for fully connected layer. Orange cube represents feature maps. Network output is a two-dimensional one-hot vector, which indicates the forecast result of input magnetogram image.
Paper: Deep Learning Based Solar Flare Forecasting Model. II. Influence of Image Resolution
Authors: Sixuan Liu, Long Xu, Zhongrui Zhao, R. Erdélyi, Marianna B. Korsós, Xin Huang
Figure caption: Examples for the magnetograms of ARs with different resolutions. This AR is NOAA 12497 on 2016 February 12. We artificially reduce the resolution of active regions to construct several databases. The resolution scale is marked in the upper right corner of the image. “1/1” represents the original magnetogram, “1/n” means downsampling the image to one nth of the original magnetogram.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: IRTF/SpeX spectra of MYSO sample. The left panels show the flux spectra with the Rayleigh–Jeans continuum of a hot star (dashed) and a blackbody continuum spectrum of warm dust (dotted), both reddened by the same amount of foreground extinction. The sum of the two components, indicated by the red line, is used to put the spectra on optical depth scale. The right panels zoom in on the M-band spectrum, on optical depth scale. A local baseline is indicated with the dashed red line, which is subtracted before the OCN−, CO, and OCS ice absorption features are analyzed.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Panel (a): peak position vs. width for the profile of the C–O stretch mode of solid OCS as a function of mixing ratio and temperature for nonirradiated mixtures, taken from Hudgins et al. (1993), Palumbo et al. (1995), and Ferrante et al. (2008). Different ice mixtures are distinguished by different symbols and colors. Mixing ratios are labeled relative to OCS (e.g., CH3OH-10 means a mixing ratio of CH3OH:OCS = 10:1). For a given ice mixture, different temperatures are connected with a line. For each temperature series, the lowest temperature mixture is indicated with an open symbol. The unlabeled dark blue squares indicate a mixture of H2O:CH3OH:OCS = 3:10:1, and the dark blue triangles of H2O:CH3OH:OCS = 100:50:1. The peak position changes typically by the amount indicated by the black arrow if the OCS is present at concentrations >10% on grains with shapes of a continuous distribution of ellipsoids, rather than on a flat surface as in the laboratory transmission spectra. The black bullets with error bars indicate the peak positions and widths observed toward the sample of MYSOs. Panel (b): similar to panel (a), but here the observations (black bullets) are compared to the proton-irradiated mixtures of Ferrante et al. (2008).
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Panel (a): distribution of the total CO ice abundance relative to H2O ice toward MYSOs. The solid black histogram is for MYSO detections presented in this work. The hatched red histogram is for all CO ice detections of previous work. Panel (b) shows the CO ice abundances toward low-mass YSOs (black) and comets (blue hatched). Panel (c) shows CO ice abundances relative to H2O ice for lines of sight tracing quiescent dense cloud material. In all panels, the unfilled histogram includes abundance upper limits. Panels (d), (e), and (f) show the abundances of CO ice in the polar phase relative to H2O ice for MYSOs, low-mass YSOs, and background stars, respectively. Panels (g), (h), and (i) show the abundances of CO ice in the apolar phase toward these same target categories.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Panel (a): distribution of the CH3OH ice abundance relative to H2O ice toward MYSOs. The solid black histogram is for MYSO detections presented in this work. The hatched red histogram is for all CH3OH ice detections of previous work. Panel (b) shows the CH3OH ice abundances toward low-mass YSOs (black) and comets (blue hatched). Panel (c) shows CH3OH ice abundances relative to H2O ice for lines of sight tracing quiescent dense cloud material. In all panels, the unfilled histogram includes abundance upper limits. Panels (d), (e), and (f) show the abundances of OCN− ice relative to H2O ice for MYSOs, low-mass YSOs, and background stars, respectively.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Distribution of the OCS ice abundance relative to H2O ice toward MYSOs (panel (a)). The solid black histogram is for MYSO detections presented in this work. The unfilled histogram includes abundance upper limits. The hatched red histogram is for all OCS ice detections of previous work. Panel (b) shows the OCS abundance in comets (Saki et al. 2020), with the open histogram including upper limits. Panel (c) shows the OCS ice abundances relative to CH3OH ice for the MYSOs presented in this (black) and previous (red) work.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Correlation plots of the OCS column density vs. that of other ice species toward MYSOs. The values in each top left corner are the Spearman’s Rank coefficient, and each second number is the significance of there being no correlation.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Correlation plots of CH3OH with OCN− (panel (a)) and COpolar (panel (b)), and of COpolar with OCN− (panel (c)), toward MYSOs. The values in each top left corner are the Spearman’s Rank coefficient, and each second number is the significance of there being no correlation.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Extraction of the CH3OH ice absorption band (solid green line) from the L-band spectra of the MYSO sample. For more details, see the caption of Figure 10.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Best fit of the NuSTAR (black) and INTEGRAL-IBIS (red) spectra with model Y. Top panel: flux-energy spectrum in units of counts per seconds per keV, both data and model. The solid lines are the total models. The nonsolid lines are the additive components: the dotted line is the background model, the dashed lines are the continuum, the dashed–dotted lines are the reflection, and the dashed–dotted–dotted lines are the high-energy tail. Bottom panel: residuals of the best fit.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Best fit of the NuSTAR (black) and INTEGRAL-IBIS (red) spectra with model 2b. Top panel: flux-energy spectrum in units of counts per seconds per keV, both data and model. The solid lines are the total models. The nonsolid lines are the additive components of the models: the dotted line is the background model, the dashed lines are the continuum, and the dashed–dotted lines are the reflection. Bottom panel: residuals of the best fit.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Best fit of the NuSTAR (black) and INTEGRAL-IBIS (red) spectra with model X. Top panel: flux-energy spectrum in units of counts per seconds per keV, both data and model. The solid lines are the total models. The nonsolid lines are the additive components: the dotted line is the background model, the dashed line is the continuum, the dashed–dotted line is the Gaussian, and the dashed–dotted–dotted line is the thermal disk. Bottom panel: residuals of the best fit.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: The Bayesian fit of the AQUAL model (Equation (6)) to all data points (left), the outer RC data points (center), and the inner RC data points (right). Blue and red points with error bars indicate the fitted values for the outer and inner parts, respectively. The difference in the fitted values of ﹩\tilde{e}﹩ for the inner and outer parts is evident, whereas the fitted a 0 values are consistent with each other. The magenta vertical line indicates the mean external field expected from the cosmic baryon distribution in the local universe (Chae et al. 2021, 2022), which is consistent only with the fitted ﹩\tilde{e}﹩ for the outer part.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: (A) Colored dots represent posterior values of stellar mass (M ⋆) and halo mass (M 200) from MCMC modeling results for three halo models. The prior relation between M ⋆ and M 200 is from the Kravtsov et al. (2018) abundance matching relation. Orthogonal residuals shown in the bottom panel indicate that the posterior median relations agree with the prior relation. (B) The MCMC results based on the prior relation between M ⋆ and M 200 from Behroozi et al. (2013). Even in this case, the posterior median relations agree better with the Kravtsov et al. (2018) abundance matching relation.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: (Upper panel) Colored dots represent posterior values of c −2(≡r 200/r −2) where r −2 is the radius where the logarithmic slope of the halo density is −2. The posterior values are compared with the NFW (Navarro et al. 1997) concentration from a ΛCDM DM-only simulation assuming the Planck cosmology (Dutton & Maccio 2014). (Lower panel) The posterior values of the ratio c −2/c NFW (where c NFW is the NFW concentration from the ΛCDM DM-only simulation) are compared with the DC14 simulations prediction (Di Cintio et al. 2014b) represented by the dashed curve. Note that the prior relation was imposed only in obtaining the DC14 MCMC results.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Posterior values of the logarithmic slope of the halo density between r = 0.01r 200 and 0.02r 200 are compared with the prediction from various cosmological hydrodynamic simulations of galaxy formation. The red band represents the uncertainty from the Maccio et al. (2020) simulations without black hole (BH) feedback. This band roughly covers the range from all previous simulations without BH feedback. The blue band represents the uncertainty for halos with M 200 ≳ 4 × 1012 M ⊙ from the Maccio et al. (2020) simulations with BH feedback.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Same as Figure 7 but for a subsample of 111 bulgeless galaxies with L < 1011 L ⊙. The difference between the inner and outer parts remains nearly the same.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Colored dots represent posterior values of three indices of the halo model given by Equation (4) from the DC14 modeling results. The bottom panel compares the posterior values with the DC14 prior values (Di Cintio et al. 2014b) represented by dashed curves.
Paper: Observational Analysis and Numerical Modeling of the Solar Wind Fluctuation Spectra during Intervals of Plasma Instability
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Sample magnetic power P  B  and magnetic helicity σ  m  spectra with a power elevation. The dashed line in the top panel is a least-squares power-law fit. The dashed line in the bottom panel shows a zero helicity value for reference.
Paper: Observational Analysis and Numerical Modeling of the Solar Wind Fluctuation Spectra during Intervals of Plasma Instability
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Same as Figure 1 but showing a sample without a power elevation.
Paper: Discovery of a Double Sequence of Blue Straggler Stars in the Core-collapsed Globular Cluster NGC 6256
Authors: Mario Cadelano, Francesco R. Ferraro, Emanuele Dalessandro, Barbara Lanzoni, Cristina Pallanca, Sara Saracino
Figure caption: Left panel: PM-cleaned CMD of NGC 6256 (gray dots) with the selected populations of 37 BSSs and 1585 reference stars highlighted in black. The solid lines draw the adopted selection boxes. The dashed line marks the threshold used to select the bright BSS sample (empty circles) for the computation of A +. Right panel: cumulative radial distributions of the 20 bright BSSs (upper line) and the 1368 reference stars (lower line) included with r hm, used to determine the A + parameter. The area of the region shaded in gray between the two cumulative radial distributions is the value of ﹩{A}_{\mathrm{rh}}^{+}﹩, which is also labeled in the panel.
Paper: Discovery of a Double Sequence of Blue Straggler Stars in the Core-collapsed Globular Cluster NGC 6256
Authors: Mario Cadelano, Francesco R. Ferraro, Emanuele Dalessandro, Barbara Lanzoni, Cristina Pallanca, Sara Saracino
Figure caption: As in Figure 7, but with models superposed. The two thick blue lines correspond to collisional isochrones (Sills et al. 2009) of 0.1 and 1 Gyr (see labels) and they well repoduce the observed BSS blue sequence. The black solid lines are standard isochrones extracted from the Dotter et al. (2008) database and computed for the cluster metallicity ([Fe/H]= −1.6) at 1 and 13 Gyr (leftmost and rightmost curves, respectively). The black dashed line corresponds to the 1 Gyr isochrone shifted in magnitude by = −0.75.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption:  K-band spectra of the NIR counterparts of the UC H II regions W51a (top spectrum), W51b1 (middle), and W51b2 (bottom). Based on the features identified in the spectra, we assigned the spectral type indicated. All spectra are continuum-normalized and were not corrected for the heliocentric velocity. The vertical dotted lines indicate typical photospheric lines used to determine the spectral type of massive stars, as much as the wavelength of 12CO and 13CO bandheads. The inset shows the double-peak profile of the Brγ line observed in the spectrum of W51b2. The horizontal axis is a velocity scale, centered at the vacuum rest wavelength of the line (vertical dotted line), and the horizontal dashed line indicates the level of the continuum in the spectrum.
Paper: Discovery of a Double Sequence of Blue Straggler Stars in the Core-collapsed Globular Cluster NGC 6256
Authors: Mario Cadelano, Francesco R. Ferraro, Emanuele Dalessandro, Barbara Lanzoni, Cristina Pallanca, Sara Saracino
Figure caption: Relation between A + and ﹩\mathrm{log}({N}_{\mathrm{relax}})﹩ (solid line) obtained by Ferraro et al. (2018) for 48 Galactic GCs (gray symbols; circles and diamonds mark “normal” and PCC clusters, respectively). The position of NGC 6256 is marked with a red diamond.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption:  K-band spectra of the NIR counterparts of the UC H II regions W51c1, W51e1, and W51e7. Based on the features identified in the spectra, we assigned the spectral type indicated. Each spectrum was normalized by its continuum, and spectra were not corrected for the heliocentric velocity. The vertical dashed lines indicate typical photospheric lines used to determine the spectral type of massive stars, as much as the wavelength of 12CO and 13CO bandheads. Emission lines in the W51c1 spectrum are artifacts introduced by the sky subtraction step.
Paper: Discovery of a Double Sequence of Blue Straggler Stars in the Core-collapsed Globular Cluster NGC 6256
Authors: Mario Cadelano, Francesco R. Ferraro, Emanuele Dalessandro, Barbara Lanzoni, Cristina Pallanca, Sara Saracino
Figure caption: Left panel: vector point diagram of the stars in common between the two HST epochs, with the black dots being the subsample of stars with magnitude 19.0 < m F555W < 22.5, and the gray dots corresponding to all the remaining stars. The upper and side plots show histograms of the PM distribution of the selected subsample along the R.A. and decl. directions, with superimposed the best-fit Gaussian function. The red circle in the main panel is centered on the mean values of the best-fit Gaussian functions (i.e., 0 mas yr−1) and has a radius of 0.6 mas yr−1, equal to the combined 2σ PM dispersion of the subsample (see text). This circle encloses all the stars that have been selected as bona-fide cluster members. Right panels: CMDs of the first-epoch data set for all the stars selected as cluster members (left) and for the stars selected as field interlopes (right).
Paper: Discovery of a Double Sequence of Blue Straggler Stars in the Core-collapsed Globular Cluster NGC 6256
Authors: Mario Cadelano, Francesco R. Ferraro, Emanuele Dalessandro, Barbara Lanzoni, Cristina Pallanca, Sara Saracino
Figure caption: PM-selected CMD of NGC 6256 zoomed into the BSS region, with the BSSs aligned along the blue and the red sequence plotted as blue and red large circles, respectively. The empty triangles mark candidate variable stars. The black line is the linear fit to the blue BSS sequence (with slope 4.7 and intercept 14.04). The distribution of the BSS distances from this line is plotted as a histogram in the inset panel.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: False-color near-infrared image of the W51 North region. The image is color-coded as red (K band), green (H band), and blue (J band) from the UKIDSS Survey (Lawrence et al. 2007), overlaid by the 6 cm radio emission contours from Mehringer (1994). The contours are placed at 3 n−σ  level (n = 1, 2, 3, ...). The UC H II regions studied in this work are labeled and indicated by the yellow circles. The map corresponds to a field of view of 8′ × 8′, centered at R.A. = 19:23:40.0, decl. = +14:30:51 (J2000).
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Distribution of our X–shooter/ALMA sample (orange diamonds) and from other z ≳ 5.7 studies (violet circles) in the black hole mass vs. bolometric luminosity plane. Filled symbols indicate that the Mg II line was used to derive the black hole mass, while empty symbols indicate the use of the C IV line. Gray contours and gray points indicate the location of SDSS DR7 0.35 < z < 2.79 quasars for which either Mg II or C IV lines were fitted by Shen et al. (2011). Diagonal gray lines mark lines of constant Eddington ratio, with dotted, dashed–dotted, and dashed lines indicating 0.01×, 0.1×, and 1× the Eddington limit, respectively. Histograms in the right and top panels are normalized to the total number of objects and follow the same color scheme as the main panel. The top and right panels also show the distribution of 0.6 ≲ z ≲ 2.3 luminosity-matched quasars as black hatched histograms.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Distribution, in the redshift vs. absolute magnitude plane, of the 38 z ≳ 5.7 quasars in our sample (orange diamonds) and of the 97 quasars for which black hole masses and Eddington ratios have been presented in the literature (violet circles; see Section 5 for details). For comparison, pale blue circles indicate all high-redshift quasars published at the time of writing (2022 May). Data for the quasar J0439+1634 (z = 6.51), that is lensed by a foreground galaxy, has been corrected by the magnification factor of ∼51 calculated by Fan et al. (2019). The horizontal dotted line marks the characteristic magnitude of z ≳ 6 quasars (﹩{M}_{1450}^{\star }\sim -25.2\,\mathrm{mag}﹩). Histograms on the top and right panels follow the same color scheme as the central panel and are normalized by the total number of objects (histograms of the quasars part of our sample and from the literature are stacked one above the other with normalization given by the total 38+97 number of objects). Most of the targets from our sample and from the literature have M 1450 ≲ −26 mag. Thus, we are probing the bright end of the underlying z ≳ 6 quasar population.